The Spectrum of Beta Lyrae

Sahade, Jorge; Huang, Su-Shu; Struve, Otto; Zebergs, V.

doi:10.2307/1005856

Cited by 36 publications

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“…Soon (astronomically) there will be no transfer of mass and consequently no increase in period or widening of separation. Actually, this tendency is already shown incipiently in the equation of observed times of light-minima (e.g., Sahade et al 1959), from which we can see that, while the third term definitely indicates the increase in period with time, the rate of increase is slowing down because of the negative sign in the fourth term.…”

Section: Evolutionary Significancementioning

confidence: 62%

An Interpretation of Beta Lyrae.

Huang¹

1963

ApJ

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bTo explain the B Lyrae system's peculiar spectroscopic and photometric behavior, a model in which the primary component is assumed to be the less massive of the two components has been constructed. Consequently, a theory of emission lines that predicts a redshifted peak superimposed on a broad emission line has been proposed. The observed shift in the y-velocity of the emission peaks is thereby understood. Finally, the evolution of the component stars leading to the present situation is discussed.

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Section: Evolutionary Significancementioning

confidence: 62%

An Interpretation of Beta Lyrae.

Huang¹

1963

ApJ

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“…1). The "narrow" component is not the same as what in an earlier paper (Sahade et al 1959) was called "emission peak," the "emission peak" being actually part of the "narrow" component (Sahade 1966). Despite the difficulties of these reconstructions, the results indicate that the central heights (or intensities) have been fairly well determined.…”

mentioning

confidence: 87%

“…This paper is largely based on results obtained during the campaign, but is not a complete report on it. Sahade et al (1959) and Sahade (1966) have already suggested that the hydrogen-line emission profiles have two components. This structure seems most obvious during eclipses.…”

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confidence: 93%

The Emission Profile of Hα in the Spectrum of β Lyrae

Batten¹,

Sahade²

1973

PASP

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The emission profile of Ha above the continuum in the spectrum of ß Lyr appears to consist of two components, a "broad" one of total width about 1000 km sec -1 and central intensity approximately equal to that of the neighboring continuum at midprimary eclipse, and a "narrow" one of total width between 600 km sec -1 and 700 km sec -1 and central intensity several times that of the broad component. The total intensity of the emission remains approximately constant over time intervals comparable to the orbital period, the large apparent changes being mainly the results of the changing intensity of the stellar continua during the eclipses. From one year to another, however, real changes in the mean emission intensity may occur.The center of the narrow component shows litde or no velocity shift throughout the orbital cycle. The center of the broad component shows shifts that could be interpreted as being opposite in phase to those shown by the primary (B8 absorption) spectrum. Preliminary measures of Hß and Hy suggest that the Balmer decrement of the narrow component is appreciably steeper than that of the broad component.A tentative explanation of these facts is offered. The narrow component of the emission is believed to arise in a shell or ring surrounding the whole system, while the broad component comes from an envelope around the still unobserved secondary star. The "satellite" lines seen in the spectrum during primary eclipse are explained as absorption lines produced in the envelope, rather than as a direct result of absorption by gaseous streams. Actually there is only one gaseous stream in the system flowing from the B8 component toward its companion.

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“…Thus the expanding shell (cloud) is given a spectral type of B2 or B5 compared with the central star's type of B8. The red-dis placed satellite lines are described as resembling an A2 spectrum (Sahade et al, 1959), or more precisely, mainly on the basis of the ratio of the intensities of the lines of Fe i to those of Fe n, intermediate in type between a Cygni (A2) and a Persei (F5) (Struve and Zebergs, 1959), while the violet-displaced satellite lines correspond to a distinctly higher stage of ionization. Thus different ionization temperatures can be assigned to the various parts of the circumstellar matter in p Lyrae, although the different sets of lines do show anomalous intensities.…”

Section: Ionization and Temperature Of Circumstellar Mattermentioning

confidence: 99%

Discussion of Observations of the Flow of Matter Within Binary Systems

Batten

1973

Symp. - Int. Astron. Union

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Observational determinations of density, dimensions, temperatures, and velocities of circumstellar features are surveyed and discussed, with a view to establishing limiting values that could be useful in any theoretical treatment of circumstellar structure. Densities of the order of 1013 particles cm-3 are found for streams and disks, although there is evidence for regions of much lower density in many systems, and some systems may have much denser circumstellar matter.Dimensions of disks seem to be remarkably constant (fractional radius ∼ 0.3) in a wide variety of systems. The total mass of circumstellar matter is always a small fraction of the mass of the system. Temperatures are usually similar to the temperatures of the stars in the system, although hot spots certainly exist in some systems, and ‘flare’ activity is evidence of localized very high temperatures. On the other hand, some systems may contain solid circumstellar matter. Observed velocities are usually several hundred km s-1. The empirical relation between the velocity of rotation of disks and the orbital period is described. Finally, the stability of these features is briefly discussed.

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The Spectrum of Beta Lyrae

Cited by 36 publications

References 0 publications

An Interpretation of Beta Lyrae.

An Interpretation of Beta Lyrae.

The Emission Profile of Hα in the Spectrum of β Lyrae

Discussion of Observations of the Flow of Matter Within Binary Systems

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